Kavli Affiliate: Alexander P. Ji
| First 5 Authors: Jennifer Mead, Kaley Brauer, Greg L. Bryan, Mordecai-Mark Mac Low, Alexander P. Ji
| Summary:
We investigate how stellar feedback from the first stars (Population III)
distributes metals through the interstellar and intergalactic medium using the
star-by-star cosmological hydrodynamics simulation, Aeos. We find that energy
injected from the supernovae of the first stars is enough to expel a majority
of gas and injected metals beyond the virial radius of halos with mass $M_*
lesssim 10^7$ M$_odot$, regardless of the number of supernovae. This prevents
self-enrichment and results in a non-monotonic increase in metallicity at early
times. Most minihalos ($M gtrsim 10^5 , rm M_odot$) do not retain
significant fractions of the yields produced within their virial radii until
they have grown to halo masses of $M gtrsim 10^7 , rm M_odot$. The loss of
metals to regions well beyond the virial radius delays the onset of enriched
star formation and extends the period that Population III star formation can
persist. We also explore the contributions of different nucleosynthetic
channels to 10 individual elements. On the timescale of the simulation (lowest
redshift $z=14.3$), enrichment is dominated by core-collapse supernovae for all
elements, but with a significant contribution from asymptotic giant branch
winds to the s-process elements, which are normally thought to only be
important at late times. In this work, we establish important mechanisms for
early chemical enrichment which allows us to apply Aeos in later epochs to
trace the evolution of enrichment during the complete transition from
Population III to Population II stars.
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